adsabs/AstroCLIMB huggingface dataset:
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Example postage stamp cutouts and stacked images for objects in the HST UVIS F336W band in the A0370 cluster. This is the same as Figure 6; however, the top row shows the F336W band, and a total of 15 galaxies are included in the stack. See the caption of Figure 6 and the text for details on the stacking methodology, with only one method demonstrated here.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: The LyC (left), UV (middle), and F814W (right) postage stamps for the two galaxies in our sample with flux measurements of >2σ in LyC. Postage stamps are ∼1.″5 × 1.″5 in size. Object ID 803 is located in the MACS 1149 cluster and detected in the F336W band at redshift z = 3.28. Source ID 809 is also detected in the F336W band and is located in the A0370 cluster field at z = 3.28
Paper: X-Ray Photoabsorption of Density-sensitive Metastable States in Ne VII, Fe XXII, and Fe XXIII 
Authors: René Steinbrügge, Steffen Kühn, Fabrizio Nicastro, Ming Feng Gu, Moto Togawa, Moritz Hoesch, Jörn Seltmann, Ilya Sergeev, Florian Trinter, Sonja Bernitt, Chintan Shah, Maurice A. Leutenegger, José R. Crespo López-Urrutia
Figure caption: Scheme of the experiment at PETRA III. The photon beam coming from the undulator passes the monochromator and is focused onto the coaxially aligned, elongated ion cloud confined inside the electron beam ion trap. Fluorescence photons emitted by the trapped ions are registered by a silicon-drift detector mounted perpendicular to the beam.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Concentration vs. asymmetry diagram for our sample of line emitters with HST morphologies. Lines denoting the typical regions where mergers and late-type galaxies are located at z = 0 are based on Bershady et al. (2000) and Conselice (2003). As can be seen, the sample is mostly divided into merger candidates and late-type galaxies.
Paper: Emission Line Galaxies in the SHARDS Hubble Frontier Fields. II. Limits on Lyman-continuum Escape Fractions of Lensed Emission Line Galaxies at Redshifts 2 < z < 3.5
Authors: Alex Griffiths, Christopher J. Conselice, Leonardo Ferreira, Daniel Ceverino, Pablo G. Pérez-González, Olga Vega, Daniel Rosa-González, Anton M. Koekemoer, Danilo Marchesini, José Miguel Rodríguez Espinosa, Lucía Rodríguez-Muñoz, Belén Alcalde Pampliega, Elena Terlevich
Figure caption: Asymmetry measurements for the galaxies described in Section 3.4 compared with signal-to-noise ratio on the y-axis and color coded by stellar mass. The dashed gray vertical line displays the threshold used to classify a source as a potential merger following Equation (6).
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Proposed full reaction path, starting from CH2CH2OH + O(3P), at the CCSD(T)/aug-cc-pVTZ//B2PLYP-D3/aug-cc-pVTZ level of theory. The relative energies are the electronic ones, as they remain equal for every deuterated and undeuterated reaction. The detailed energies are given in Appendix A (Tables 3–5).
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Structures of the various isotopomers of 2-hydroxylethyl radical, (first column) of the relative addition RI1 (second column), of the TS2 connecting RI1 and the products (fourth column), and of the resulting isotopomers of glycolaldehyde (last column) for reactions 5 through 9. The D atoms are marked in orange.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Unimolecular rate coefficients from RI1 to cis-glycoaldehyde via TS2. Red: all-protium reaction. Green: CH2ODCHO from reaction 5. Blue: CHDOHCHO from reaction 6. Magenta: CHDOHCHO from reaction 7. Light blue: CH2OHCDO from reaction 8a. Purple: CH2OHCDO from reaction 9a.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Different types of deuterated ethanol (left) and deuterated 2-hydroxyethyl radical (CH2CH2OH; right).
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Loop of deuteration regarding reaction 5.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Loop of deuteration regarding reaction 2.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Loop of deuteration regarding reaction 4.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Loop of deuteration regarding reaction 1.
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Loop of deuteration regarding reaction 3.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Comparison between the amplitude of a BNS signal analogous to GW170817, as seen by a single instrument of the ET triangular detector (whose sensitivity curve is shown in green) accounting for the effect of Earth's rotation (violet curve) and without accounting for it (orange curve). The dashed vertical lines indicate the amount of time left before coalescence, and the amplitude is computed using the waveform model IMRPhenomD_NRTidalv2. For comparison, we also report in blue a representative LIGO Livingston sensitivity curve during the second observing run, available at.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Noise amplitude spectral densities, ASDs, of the various detectors considered. To have a uniform comparison between different geometries, the single-detector ET sensitivity curve has been rescaled by a factor 2/3 to take into account that, having a triangular design, ET actually consists of 3 nested instruments with an opening angle of 60°.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Scatter plot of the condition numbers of the Fisher matrices as a function of the system inclination angle, computed for BBH events detected at a network consisting of ET+2CE, using the IMRPhenomHM waveform model. In the left panel, we report on the color bar the inversion errors associated with the events; and in the central panel, the S/Ns; and in the right panel, the relative errors on the luminosity distance. The horizontal dashed line shows the inverse machine precision limit, of 1015.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Distribution of the quenched fraction of the Horizon-AGN galaxies. The horizontal axis is the host halo mass, and the vertical axis is the stellar mass of member galaxies. The black numbers are quenched fractions color-coded following the key at the bottom and the white numbers are central galaxy fractions. The mean values of the quenched fractions of field galaxies are shown in the gray inset. The top and right panels show the number distributions of the host halos and their member galaxies, respectively. Note that there are only two halos (clusters) of mass M halo ≥ 1014.5  M ⊙ because of the limited volume of Horizon-AGN (140 Mpc on a side).
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Phase-space diagram of Horizon-AGN group/cluster member candidates in the last snapshot (z = 0.018). The horizontal axis is the distance of the galaxy from the center of the host halo normalized by the virial radius of the halo. The vertical axis is the relative velocity of the galaxy normalized by the circular velocity. The black line indicates the relative velocity threshold of Han et al. (2018) for selecting satellites. Gray points are galaxies not identified as members, and other color scales show the time since infall of member galaxies (Section 2.2).
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Mean SFHs of the Horizon-AGN galaxies of different masses. Other mass bins not shown here are presented in Appendix A. Different colors and line styles represent the different classifications of environments, and the number of galaxies for each subsample is indicated in brackets. The group galaxies (green) mean the galaxies in the host halos of mass 1013−14  M ⊙ and the cluster galaxies (red) are in the halos more massive than 1014  M ⊙. The shaded area shows the 1σ standard deviation. All the lines are smoothed using a Savitzky–Golay filter and a Gaussian kernel.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: Distribution of the e-folding timescales (τ) of field galaxies in the Horizon-AGN simulation. The grayscale histogram shows the column-normalized number density, and the white contours show the number of galaxies with labels marked. The median values are presented for four mass bins.
Paper: Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation
Authors: Seyoung Jeon, Sukyoung K. Yi, Yohan Dubois, Aeree Chung, Julien Devriendt, San Han, Ryan A. Jackson, Taysun Kimm, Christophe Pichon, Jinsu Rhee
Figure caption: SFHs (the shaded area) of four sample Horizon-AGN galaxies and fits using Equation (5) (the lines). The different colors and line styles represent the cases of τ ∼ 1, 2, 4, and 10.6 Gyr, respectively. Each line and shaded area are normalized to the integrated SFR for clarity.
Paper: Radio Pulse Profiles and Polarization of the Terzan 5 Pulsars
Authors: Ashley R. Martsen, Scott M. Ransom, Megan E. DeCesar, Paulo C. C. Freire, Jason W. T. Hessels, Anna Y. Q. Ho, Ryan S. Lynch, Ingrid H. Stairs, Yuankun Wang
Figure caption: Summed profiles for 32 of the L-band (covering roughly 1150−1850 MHz) profiles for the Terzan 5 pulsars. The remaining pulsars are not shown due to very low signal-to-noise, or complications that kept them from being summed. The profile from Ter5A is from a single observation (see the text). The black lines are total intensity, red lines are the linear polarization L with the mean L off-pulse subtracted, and the blue is the circular polarization V in the IAU/IEEE convention. The position angle is shown above each profile if it is 3σ significant, resulting in some anomalous “detections” due to noise even in off-pulse portions of the profiles. The primary y-axis scales (in flux density, mJy), are different for each pulsar.
Paper: Radio Pulse Profiles and Polarization of the Terzan 5 Pulsars
Authors: Ashley R. Martsen, Scott M. Ransom, Megan E. DeCesar, Paulo C. C. Freire, Jason W. T. Hessels, Anna Y. Q. Ho, Ryan S. Lynch, Ingrid H. Stairs, Yuankun Wang
Figure caption: Map of the projected average parallel component of the Galactic magnetic field strength toward Terzan 5, centered on the optical position of the cluster, with the core radius shown as a black circle (Lanzoni et al. 2010). The gray arrow points to the Galactic center, which is 4.°19 in that direction, and the gray line through the center of the cluster is parallel to the Galactic plane. The color bar indicates 〈B ∣∣〉 in μG toward each pulsar, from the lowest value to the second highest. These values were calculated using the rotation measures (RMs) as determined by rmfit (see Table 1). We omitted Ter5aa since the RM values determined by the two different methods are inconsistent, and grayed-out Ter5D since it has a significantly higher RM (and therefore 〈B ∣∣〉) than the rest of the pulsars, ∼1.18 μG. There is an obvious gradient in 〈B ∣∣〉 roughly in the R.A. direction.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Changes in the accretion rate (﹩\dot{M}﹩), the outflow power (P out), the total angular momentum flux (﹩{\dot{J}}_{\mathrm{int}}^{r}﹩), the ratio between the shell-integrated Maxwell and advective fluxes (﹩{\dot{J}}_{\mathrm{stress},{\rm{M}}}^{r}/{\dot{J}}_{\mathrm{adv}}^{r}﹩), and the Reynolds stress (α R) are correlated in MADs. We show the time–radius plot for each quantity for the MAD model. The white regions in ﹩\dot{M}﹩ indicate a net outward mass flux. The dashed lines in the ﹩\dot{M}﹩ panel indicate time snapshots over which we track one magnetic flux eruption event in Figure 19. ﹩{\dot{J}}_{\mathrm{adv}}^{r}﹩ is generally directed inward toward the BH, and so we use a negative sign for the ratio calculation. White regions in the ﹩{\dot{J}}_{\mathrm{stress},{\rm{M}}}^{r}/{\dot{J}}_{\mathrm{adv}}^{r}﹩ plot indicate a net outward angular momentum flux due to advection.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We compare the gas density profiles of the accretion flows in Sgr A* and M87* with the MAD and SANE models (from Figure 6). The observational data and the simulations show consistent radial profiles: ∼ρ ∝ r −1. We take the horizon-scale densities from Event Horizon Telescope Collaboration et al. (2019, 2022) and the Bondi-scale data from Figure 6 of Alexander et al. (2016), originally from Baganoff et al. (2003) for Sgr A* and from Russell et al. (2015) for M87*. The dashed lines indicate power-law fits connecting the near-horizon data points with the Bondi-scale data.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Magnetic flux eruptions trigger strong disk winds and drive outward angular momentum transport in MADs. We show the midplane and vertical cross sections of the gas density ρ and the radial and polar fluxes of the angular momentum at three different times corresponding to the dashed lines in Figure 18, tracking the evolution of a particular flux eruption. The dashed lines in the first column indicate the azimuthal angle at which we take the corresponding vertical slice. The blue (red) regions indicate outward (inward) fluxes for ﹩{T}_{\varphi }^{r}﹩ and clockwise (counterclockwise) fluxes for ﹩{T}_{\varphi }^{\theta }﹩. Flux eruptions push gas outward, creating outward fluxes as seen from the right halves of the vertical slices. The left halves of these plots show a region of the disk that does not have a flux eruption. Hence, turbulence drives a net inward transport of angular momentum, similar to that in a SANE disk.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the shell-integrated components of the radial flux of angular momentum (from Figures 10 and 13) for the MAD (left) and SANE (right) simulations, time-averaged over the final 50,000r g/c. Solid (dashed) lines indicate outward (inward) transport. Maxwell stresses dominate the outward angular momentum flux for both models, but it is so strong for the MAD model that it matches the inward advective flux, showcasing the importance of magnetic fields in regulating angular momentum transport in MADs.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: The MAD simulation exhibits an outward vertical flux of angular momentum caused by stresses, while the SANE disks are dominated by equatorial flux. Top: A schematic diagram showing the calculation of the net ﹩{\dot{J}}_{\mathrm{stress}}﹩ for an annulus within the disk. The black dashed lines indicate h/r. Bottom: We show the ratio between the net outward angular momentum fluxes due to fluid stresses in the polar and radial directions. Solid (dashed) lines correspond to a net positive (negative) ratio, and indicate the direction of the net polar flux. In the MAD model, the outward polar flux is as strong as the outward radial flux, consistent with the result in Figure 11. In contrast, the SANE model has a weak polar influx of angular momentum at r ≳ 20r g.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: We show the time-averaged α viscosity parameters for both models: the Maxwell stress α M, the Reynolds stress α R, and the net value of α R + α M. Solid (dashed) lines indicate outward (inward) stresses. The MAD model exhibits an inward Reynolds stress, which results in the inward transport of angular momentum as seen in Figure 14.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: The centrifugal force and thermal pressure generally support the disk while magnetic forces dominate the wind. We show the different radial forces due to the thermal pressure, magnetic fields, and gravity for the MAD model. Top: Radial forces at radius r = 20r g, calculated over the time period 2.4–2.9 × 105 r g/c. The vertical dotted lines show the disk scale aspect ratio h/r at 20r g. Bottom: Radial profile of disk-averaged forces. We see that the poloidal magnetic tension dominates the total magnetic force in the disk at least for r ≲ 20r g.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Same as Figure 10, but for the Maxwell and Reynolds components of the stress-induced angular momentum flux, ﹩{\dot{J}}_{\mathrm{stress},{\rm{M}}}﹩ and ﹩{\dot{J}}_{\mathrm{stress},{\rm{R}}}﹩. The Maxwell component dominates and thus, the streamlines look similar to those of the total ﹩{\dot{J}}_{\mathrm{stress}}﹩. An important feature shown here is that ﹩{\dot{J}}_{\mathrm{stress},{\rm{R}}}﹩ points inward for the MAD model while it points outward for the SANE model.
Paper: Flux Eruption Events Drive Angular Momentum Transport in Magnetically Arrested Accretion Flows
Authors: K. Chatterjee, R. Narayan
Figure caption: Here we show the angular dependence of the ﹩\dot{M}﹩-normalized angular momentum flux components at different radii—20r g, 40r g, and 60r g—with the vertical lines indicating the disk scale aspect ratio at each radius. We see a clear outward flux in the wind region of the MAD model (left column), which is in contrast to the SANE model (right column), where the fluxes are at their maximum in the disk bulk.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: The upper and lower two panels show the model fits assuming a linear (﹩\delta \mu (z)={\hat{{\rm{\Gamma }}}}_{1}z﹩) and a logarithmic (﹩\delta \mu (z)=\hat{k}\mathrm{ln}(1+z)﹩) systematic evolution of the SN Ia distances, respectively. The left and right panels are for the ΛCDM and flat w 0 w  a CDM models, respectively. The gray contours are for binned Pantheon data only, and the red for the joint data set including the VHZ SNe Ia. The contours with decreasing color weights are the 1σ, 2σ, and 3σ confidence regions.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: From the upper left clockwise, the panels show the constraints on Ω m , w 0, and w  a  of the flat w 0 w  a CDM model with the Planck 2018 measurements and the statistical errors of the Pantheon binned data reduced by a factor of 1, 2, ﹩\sqrt{8}﹩ and 8. The gray contours show the confidence levels constrained by the Pantheon binned data only, and the orange contours show those with the inclusion of the VHZ SNe Ia. The gray and orange vertical dashed lines show the 1σ confidence levels of the Pantheon binned data only and those of the combined data, respectively. The numbers of the image titles show the 1σ confidence of the combined data. The contour levels are 1σ, 2σ, and 3σ with decreasing color weight.
Paper: Constraints on Cosmological Parameters with a Sample of Type Ia Supernovae from JWST
Authors: Jia Lu, Lifan Wang, Xingzhuo Chen, David Rubin, Saul Perlmutter, Dietrich Baade, Jeremy Mould, Jozsef Vinko, Enikő Regős, Anton M. Koekemoer
Figure caption: The parameter constraints for the ΛCDM and flat w 0 w  a CDM models assuming a linear systematic evolution (﹩\delta \mu ={\hat{{\rm{\Gamma }}}}_{1}z﹩) of the SN distance modulus with redshifts for the Pantheon-only data (gray) and the joint data including the VHZ SNe (blue). The vertical dashed lines show the 1σ confidence levels. The contour levels with decreasing color weights are the 1σ, 2σ, and 3σ confidence regions.